Download Astronomy 103 Exam 2 Review

Astronomy
103
Exam
2
Review
Spring
2009
Which
star
is
ho=er,
a
G4
main
sequence
star
or
a
G4
giant?
A.  The
main
sequence
star
B.  The
giant
C.  Both
have
the
same
temperature
D.  Cannot
be
determined
from
informaLon
given
Which
star
is
ho=er,
a
G4
main
sequence
star
or
a
G4
giant?
A.  The
main
sequence
star
B.  The
giant
C.  Both
have
the
same
temperature
D.  Cannot
be
determined
from
informaLon
given
What
would
be
an
immediate
indicator
the
Sun
had
stopped
fusing
hydrogen?
A.
The
light
we
see
would
shiN
wavelengths
into
the
ultraviolet.
B.
The
Sun
would
blow
off
its
outer
layers
as
a
planetary
nebula.
C.
Solar
observatories
would
see
that
the
Sun’s
core
was
rapidly
shrinking.
D.
The
amount
of
neutrinos
observed
from
the
Sun
would
suddenly
change.
What
would
be
an
immediate
indicator
the
Sun
had
stopped
fusing
hydrogen?
A.
The
light
we
see
would
shiN
wavelengths
into
the
ultraviolet.
B.
The
Sun
would
blow
off
its
outer
layers
as
a
planetary
nebula.
C.
Solar
observatories
would
see
that
the
Sun’s
core
was
rapidly
shrinking.
D.
The
amount
of
neutrinos
observed
from
the
Sun
would
suddenly
change.
A
helium
flash:
A.  Occurs
to
all
stars
B.  Occurs
only
if
the
star’s
core
is
degenerate
C.  Creates
a
planetary
nebula
D.  None
of
the
above
A
helium
flash:
A.  Occurs
to
all
stars
B.  Occurs
only
if
the
star’s
core
is
degenerate
C.  Creates
a
planetary
nebula
D.  None
of
the
above
The
main
sequence
is:
A.  The
most
stable
phase
of
a
star’s
life
B.  Where
stars
fuse
hydrogen
into
helium
in
their
cores
C.  ComparaLvely
shorter
for
higher
mass
stars
D.  All
of
the
above
The
main
sequence
is:
A.  The
most
stable
phase
of
a
star’s
life
B.  Where
stars
fuse
hydrogen
into
helium
in
their
cores
C.  ComparaLvely
shorter
for
higher
mass
stars
D.  All
of
the
above
What
is
the
heaviest
element
that
fusion
can
produce
in
the
cores
of
massive
stars?
A.  Helium
B.  Silicon
C.  Iron
D.  Uranium
What
is
the
heaviest
element
that
fusion
can
produce
in
the
cores
of
massive
stars?
A.  Helium
B.  Silicon
C.  Iron
D.  Uranium
White
dwarfs
shine
due
to
A.  Hydrogen
shell
burning
B.  Core
fission
of
heavy
elements
C.  ReflecLon
of
light
from
their
companion
star
in
a
binary
system
D.  None
of
the
above
White
dwarfs
shine
due
to
A.  Hydrogen
shell
burning
B.  Core
fission
of
heavy
elements
C.  ReflecLon
of
light
from
their
companion
star
in
a
binary
system
D.  None
of
the
above
Protostars
can
best
be
observed
in
the
A.  Ultraviolet
B.  Infrared
C.  Visible
D.  X‐ray
Protostars
can
best
be
observed
in
the
A.  Ultraviolet
B.  Infrared
C.  Visible
D.  X‐ray
Which
of
these
star
clusters
is
the
oldest?
A.
B.
C.
D.
They
all
have
the
same
age
Which
of
these
star
clusters
is
the
oldest?
A.
B.
C.
D.
They
all
have
the
same
age
Not
all
visual
binaries
have
observed
Doppler
shiNs.
Why?
A.  Some
will
be
at
an
angle
where
the
stars
are
never
moving
directly
toward
or
away
from
Earth.
B.  Some
binary
systems
are
staLonary
C.  Some
binary
systems
have
very
ellipLcal
orbits
D.  All
of
the
above
Not
all
visual
binaries
have
observed
Doppler
shiNs.
Why?
A.  Some
will
be
at
an
angle
where
the
stars
are
never
moving
directly
toward
or
away
from
Earth.
B.  Some
binary
systems
are
staLonary
C.  Some
binary
systems
have
very
ellipLcal
orbits
D.  All
of
the
above
The
net
result
of
the
p‐p
chain
is
that
__
hydrogen
are
turned
into
__
helium
A.  1;
2
B.  3;
2
C.  4;
1
D.  4;
2
The
net
result
of
the
p‐p
chain
is
that
__
hydrogen
are
turned
into
__
helium
A.  1;
2
B.  3;
2
C.  4;
1
D.  4;
2
The
reddest
stars
spend
the
most
Lme
on
the
main
sequence
because
A.  They
are
the
most
massive
stars
and
have
more
hydrogen
fuel
B.  Their
core
pressure
and
temperature
are
low
so
the
rate
of
hydrogen
fusion
is
low
C.  They
are
fully
convecLve
D.  B
and
C
The
reddest
stars
spend
the
most
Lme
on
the
main
sequence
because
A.  They
are
the
most
massive
stars
and
have
more
hydrogen
fuel
B.  Their
core
pressure
and
temperature
are
low
so
the
rate
of
hydrogen
fusion
is
low
C.  They
are
fully
convecLve
D.  B
and
C
Why
do
we
use
Type
Ia
supernovae
to
make
distance
measurements?
A.  They
all
happen
at
the
same
distance
from
Earth
B.  The
ones
nearer
to
us
are
more
luminous
C.  They
all
have
the
same
mass
and
leave
no
remnant
D.  All
of
the
above
Why
do
we
use
Type
Ia
supernovae
to
make
distance
measurements?
A.  They
all
happen
at
the
same
distance
from
Earth
B.  The
ones
nearer
to
us
are
more
luminous
C.  They
all
have
the
same
mass
and
leave
no
remnant
D.  All
of
the
above
GranulaLon
on
the
photosphere
of
the
Sun
is
the
result
of
A.  Dust
parLcles
in
the
photosphere
B.  DistorLon
caused
by
light
passing
through
the
turbulent
solar
atmosphere
C.  MoLons
of
large
amounts
of
gas
moving
out
from
the
interior
of
the
Sun
and
then
back
in
D.  The
Sun’s
magneLc
field
GranulaLon
on
the
photosphere
of
the
Sun
is
the
result
of
A.  Dust
parLcles
in
the
photosphere
B.  DistorLon
caused
by
light
passing
through
the
turbulent
solar
atmosphere
C.  MoLons
of
large
amounts
of
gas
moving
out
from
the
interior
of
the
Sun
and
then
back
in
D.  The
Sun’s
magneLc
field
If
black
holes
emit
no
light,
how
can
we
observe
them?
Which
of
the
following
observaLon
methods
is
not
valid?
A.
Ma=er
pulled
off
a
companion
star
emits
a
characterisLc
X‐
ray
spectrum
as
it
falls
toward
the
black
hole.
B.
Companion
stars
suddenly
disappear
from
view
as
they
plunge
into
the
black
hole.
C.
Black
holes
can
act
as
gravitaLonal
lenses,
forming
mulLple
images
of
objects
beyond
the
hole.
D.
A
star
that
wobbles
in
its
proper
moLon
can
be
exhibiLng
evidence
of
its
orbital
moLon
around
an
unseen
companion.
If
black
holes
emit
no
light,
how
can
we
observe
them?
Which
of
the
following
observaLon
methods
is
not
valid?
A.
Ma=er
pulled
off
a
companion
star
emits
a
characterisLc
X‐
ray
spectrum
as
it
falls
toward
the
black
hole.
B.
Companion
stars
suddenly
disappear
from
view
as
they
plunge
into
the
black
hole.
C.
Black
holes
can
act
as
gravitaLonal
lenses,
forming
mulLple
images
of
objects
beyond
the
hole.
D.
A
star
that
wobbles
in
its
proper
moLon
can
be
exhibiLng
evidence
of
its
orbital
moLon
around
an
unseen
companion.
The
internal
structure
of
the
Sun,
from
the
center
to
the
surface
is
A.  Energy‐generaLng
core,
radiaLve
region,
convecLon
region
B.  Energy‐generaLng
core,
convecLve
region,
radiaLve
region
C.  ConvecLve
core,
chemically
reacLng
region,
radiaLve
region
D.  Energy‐generaLng
core,
convecLve
region
The
internal
structure
of
the
Sun,
from
the
center
to
the
surface
is
A.  Energy‐generaLng
core,
radiaLve
region,
convecLon
region
B.  Energy‐generaLng
core,
convecLve
region,
radiaLve
region
C.  ConvecLve
core,
chemically
reacLng
region,
radiaLve
region
D.  Energy‐generaLng
core,
convecLve
region
Which
of
these
spectral
classes
correspond
to
the
reddest
stars?
A.  O
B.  F
C.  A
D.  G
Which
of
these
spectral
classes
correspond
to
the
reddest
stars?
A.  O
B.  F
C.  A
D.  G
On
an
H‐R
diagram
a
star
is
found
to
be
evolving
to
the
right
at
a
constant
luminosity.
We
know
that
the
star
is
becoming
A.  Only
larger
B.  Only
smaller
C.  Both
smaller
and
cooler
D.  Both
larger
and
cooler
On
an
H‐R
diagram
a
star
is
found
to
be
evolving
to
the
right
at
a
constant
luminosity.
We
know
that
the
star
is
becoming
A.  Only
larger
B.  Only
smaller
C.  Both
smaller
and
cooler
D.  Both
larger
and
cooler
The
difference
between
Type
Ia
and
Type
II
supernova
is
A.  Their
masses
B.  Their
ages
C.  Their
chemical
composiLons
D.  All
of
the
above
The
difference
between
Type
Ia
and
Type
II
supernova
is
A.  Their
masses
B.  Their
ages
C.  Their
chemical
composiLons
D.  All
of
the
above
The
mechanism
that
results
in
high
rotaLon
rates
for
certain
pulsars
is
probably
A.
mass
exchange
with
a
binary
companion.
B. collapse
of
the
neutron
star,
similar
to
the
way
that
a
skater
increases
rotaLon
in
a
spin.
C. mass
loss
from
the
neutron
star,
the
remainder
spinning
faster
as
a
result.
D.
the
merger
of
a
pair
of
neutron
stars
to
form
a
single
object.
The
mechanism
that
results
in
high
rotaLon
rates
for
certain
pulsars
is
probably
A.
mass
exchange
with
a
binary
companion.
B. collapse
of
the
neutron
star,
similar
to
the
way
that
a
skater
increases
rotaLon
in
a
spin.
C. mass
loss
from
the
neutron
star,
the
remainder
spinning
faster
as
a
result.
D.
the
merger
of
a
pair
of
neutron
stars
to
form
a
single
object.
When
material
transfers
from
a
companion
to
a
white
dwarf,
we
normally
see
a
A.  Supernova
B.  Nova
C.  X‐ray
burster
D.  Gamma‐ray
burster
When
material
transfers
from
a
companion
to
a
white
dwarf,
we
normally
see
a
A.  Supernova
B.  Nova
C.  X‐ray
burster
D.  Gamma‐ray
burster
Two
observers
have
two
clocks,
one
at
rest
on
the
Earth’s
surface
and
one
at
rest
high
above
the
Earth’s
surface.
Which
statement
is
correct?
A. Each
observer
will
see
the
other's
clock
to
be
running
slow
with
respect
to
the
observer's
own
clock.
B. Each
observer
will
see
the
other's
clock
to
be
running
fast
with
respect
to
the
observer's
own
clock.
C. Both
observers
agree:
since
the
clocks
are
not
moving
with
respect
to
each
other
the
clocks
run
at
the
same
speed
and
read
the
same
Lme.
D. Both
observers
agree:
the
clock
near
Earth
is
running
slower
than
the
clock
high
above
Earth's
surface.
Two
observers
have
two
clocks,
one
at
rest
on
the
Earth’s
surface
and
one
at
rest
high
above
the
Earth’s
surface.
Which
statement
is
correct?
A. Each
observer
will
see
the
other's
clock
to
be
running
slow
with
respect
to
the
observer's
own
clock.
B. Each
observer
will
see
the
other's
clock
to
be
running
fast
with
respect
to
the
observer's
own
clock.
C. Both
observers
agree:
since
the
clocks
are
not
moving
with
respect
to
each
other
the
clocks
run
at
the
same
speed
and
read
the
same
Lme.
D. Both
observers
agree:
the
clock
near
Earth
is
running
slower
than
the
clock
high
above
Earth's
surface.
Which
of
the
following
evoluLonary
phases
are
in
order
from
youngest
to
oldest?
A.
Protostar,
red
giant,
main
sequence,
white
dwarf
B.
Protostar,
main
sequence,
white
dwarf,
neutron
star
C.
Protostar,
main
sequence,
red
giant,
white
dwarf
D.
Protostar,
planetary
nebula,
main
sequence,
supernova
Which
of
the
following
evoluLonary
phases
are
in
order
from
youngest
to
oldest?
A.
Protostar,
red
giant,
main
sequence,
white
dwarf
B.
Protostar,
main
sequence,
white
dwarf,
neutron
star
C.
Protostar,
main
sequence,
red
giant,
white
dwarf
D.
Protostar,
planetary
nebula,
main
sequence,
supernova
A
planetary
nebula
is:
A.  The
progenitor
of
a
solar
system
B.  What
remains
when
a
white
dwarf
explodes
as
a
supernova
C.  A
shell
of
gas
ejected
from
a
star
late
in
its
life
D.  The
cloud
from
which
protostars
form
A
planetary
nebula
is:
A.  The
progenitor
of
a
solar
system
B.  What
remains
when
a
white
dwarf
explodes
as
a
supernova
C.  A
shell
of
gas
ejected
from
a
star
late
in
its
life
D.  The
cloud
from
which
protostars
form
The
stars
Capella,
Aldebaran,
and
Regulus
have
parallax
angles
of
0.079,
0.05,
and
0.041
arcsec,
respecLvely.
Which
star
is
the
farthest
away?
A.  Capella
B.  Aldebaran
C.  Regulus
D.  Cannot
be
determined
from
informaLon
given
The
stars
Capella,
Aldebaran,
and
Regulus
have
parallax
angles
of
0.079,
0.05,
and
0.041
arcsec,
respecLvely.
Which
star
is
the
farthest
away?
A.  Capella
B.  Aldebaran
C.  Regulus
D.  Cannot
be
determined
from
informaLon
given
Why
are
there
no
stars
of
less
massive
than
approximately
0.08
solar
masses?
A.  They
are
sLll
contracLng
and
haven’t
yet
reached
the
main
sequence
B.  They
cannot
compress
their
cores
to
hydrogen
fusion
temperatures
C.  Their
mass
is
so
small
that
deuterium
fusion
blasts
them
apart
D.  None
of
the
above
Why
are
there
no
stars
of
less
massive
than
approximately
0.08
solar
masses?
A.  They
are
sLll
contracLng
and
haven’t
yet
reached
the
main
sequence
B.  They
cannot
compress
their
cores
to
hydrogen
fusion
temperatures
C.  Their
mass
is
so
small
that
deuterium
fusion
blasts
them
apart
D.  None
of
the
above
For
main
sequence
stars,
as
temperature
increases
A.  Mass
increases
B.  Radius
decreases
C.  Luminosity
decreases
D.  None
of
the
above
For
main
sequence
stars,
as
temperature
increases
A.  Mass
increases
B.  Radius
decreases
C.  Luminosity
decreases
D.  None
of
the
above
The
Sun
is
supported
against
the
force
of
its
own
gravity
by
A.  Gas
pressure
B.  The
force
exerted
by
escaping
neutrinos
C.  Forces
from
magneLc
fields
D.  Rapid
rotaLon
The
Sun
is
supported
against
the
force
of
its
own
gravity
by
A.  Gas
pressure
B.  The
force
exerted
by
escaping
neutrinos
C.  Forces
from
magneLc
fields
D.  Rapid
rotaLon